Fig. 2.
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Theoretical comparison between the galaxy-shear CGg(ℓ), galaxy-IA CIg(ℓ) and shear-magnification gmagCGκgal(ℓ) angular power spectra, with the best fit of our baseline analysis and the redshift distribution n(z) from KiDS-1000 0.5 < zP < 1.2 shear catalog. The dashed lines represent negative signals. This figure demonstrates that the magnification contamination is important in the self-calibration method for the high-z KiDS source sample.
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